The Discovery and Nature of the Optical Transient Css100217:102913+404220∗,†
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The Astrophysical Journal, 735:106 (21pp), 2011 July 10 doi:10.1088/0004-637X/735/2/106 C 2011. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE DISCOVERY AND NATURE OF THE OPTICAL TRANSIENT CSS100217:102913+404220∗,† A. J. Drake1, S. G. Djorgovski1, A. Mahabal1, J. Anderson2,R.Roy3, V. Mohan4, S. Ravindranath4, D. Frail5, S. Gezari6, James D. Neill1,L.C.Ho7, J. L. Prieto7, D. Thompson8, J. Thorstensen9, M. Wagner8, R. Kowalski10, J. Chiang11, J. E. Grove12, F. K. Schinzel13,D.L.Wood12, L. Carrasco14, E. Recillas14, L. Kewley15, K. N. Archana16,17, Aritra Basu17, Yogesh Wadadekar17, Brijesh Kumar3, A. D. Myers18, E. S. Phinney1, R. Williams1, M. J. Graham1, M. Catelan19, E. Beshore10, S. Larson10, and E. Christensen20 1 California Institute of Technology, 1200 E. California Blvd., CA 91225, USA 2 STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA 3 Aryabhatta Research Institute of Observational Sciences, Manora Peak, Nainital 263129, Uttarakhand, India 4 IUCAA, Postbag 4, Ganeshkhind, Pune 411007, India 5 NRAO, Campus Building 65, 949 North Cherry Avenue, Tucson, AZ 85721-0655, USA 6 Department of Physics & Astronomy, Johns Hopkins University, 366 Bloomberg Center, 3400 N. Charles Street, Baltimore, MD 21218, USA 7 Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA 8 LBT, University of Arizona, 933 N. Cherry Ave, Room 552, Tucson, AZ 85721, USA 9 Dartmouth College, 6127 Wilder Laboratory, Hanover, NH 03755-3528, USA 10 Department of Planetary Sciences, Lunar and Planetary Laboratory, The University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA 11 W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, SLAC National Accelerator Laboratory, Stanford University, Standford, CA 94305, USA 12 Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA 13 Max-Planck-Institut fur¨ Radioastronomie, Auf dem Hugel¨ 69, 53121 Bonn, Germany 14 INAOE, Tonantzintla, Puebla, Mexico 15 IFA, 640 North A’ohoku Place, #209, Hilo, HI 96720-2700, USA 16 School of Computer Sciences, Mahatma Gandhi University, Kottayam 686560, India 17 National Centre for Radio Astrophysics, TIFR, Post Bag 3, Ganeshkhind, Pune 411007, India 18 Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA 19 Departamento de Astronom´ıa y Astrof´ısica, Pontificia Universidad Catolica´ de Chile, Av. Vicuna˜ Mackena 4860, 782-0436 Macul, Santiago, Chile 20 Gemini Observatory, Casilla 603, La Serena, CL, Chile Received 2010 December 17; accepted 2011 April 26; published 2011 June 22 ABSTRACT We report on the discovery and observations of the extremely luminous optical transient CSS100217:102913+404220 (CSS100217 hereafter). Spectroscopic observations showed that this transient was coincident with a galaxy at red- shift z = 0.147 and reached an apparent magnitude of V ∼ 16.3. After correcting for foreground Galactic extinction we determine the absolute magnitude to be MV =−22.7 approximately 45 days after maximum light. Over a period of 287 rest-frame days, this event had an integrated bolometric luminosity of 1.3 × 1052 erg based on time-averaged bolometric corrections of ∼15 from V- and R-band observations. Analysis of the pre-outburst Sloan Digital Sky Survey (SDSS) spectrum of the source shows features consistent with a narrow-line Seyfert 1 galaxy. High-resolution Hubble Space Telescope and Keck follow-up observations show that the event occurred within 150 pc of the nucleus of the galaxy, suggesting a possible link to the active nuclear region. However, the rapid outburst along with photometric and spectroscopic evolution are much more consistent with a luminous supernova. Line diagnostics suggest that the host galaxy is undergoing significant star formation. We use extensive follow-up of the event along with archival Catalina Sky Survey NEO search and SDSS data to investigate the three most likely sources of such an event: (1) an extremely luminous supernova, (2) the tidal disruption of a star by the massive nuclear black hole, and (3) variability of the central active galactic nucleus (AGN). We find that CSS100217 was likely an extremely luminous Type IIn supernova and occurred within the range of the narrow-line region of an AGN. We discuss how similar events may have been missed in past supernova surveys because of confusion with AGN activity. Key words: galaxies: active – galaxies: nuclei – galaxies: stellar content – supernovae: general Online-only material: color figures 1. INTRODUCTION vational frontier has fueled the advent of the new generation of digital synoptic sky surveys, which cover the sky many times, Exploration of the time domain is now one of the most rapidly as well as the necessity of using robotic telescopes to respond growing and exciting areas of astrophysics. This vibrant obser- rapidly to transient events (Paczynski 2000). However, the dis- covery of transient astronomical events is by no means new to ∗ Some of the data presented herein were obtained at the W. M. Keck astronomy with phenomena such as supernovae being discov- Observatory, which is operated as a scientific partnership among the California ered and documented for centuries (Zhao et al. 2006). Transient Institute of Technology, the University of California, and the National events themselves have been observed on timescales from sec- Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. onds; e.g., gamma-ray bursts (GRBs; Klebesadel et al. 1973), † Based on observations made with the NASA/ESA Hubble Space Telescope, to years; e.g., supernovae (Rest et al. 2011) and active galactic obtained at the Space Telescope Science Institute, which is operated by the nuclei (AGNs; Ulrich et al. 1997). Predictions of new types of Association of Universities for Research in Astronomy, Inc., under NASA observable astrophysical phenomena continue to be theorized contract NAS 5-26555. These observations are associated with program 12117. 1 The Astrophysical Journal, 735:106 (21pp), 2011 July 10 Drake et al. and made detectable by advancing technology. For example, services such as DataScope.22 Events that remain a poor match the possibility that Massive Compact Halo Objects could be for known types phenomena are of particular interest and are observable due to gravitational microlensing was theorized by the most closely scrutinized. Paczynski (1986) and soon proven by Alcock et al. (2003) and Aubourg et al. (1993). Such discoveries set the stage for larger 2. THE DISCOVERY OF CSS100217 time domain surveys with broader goals. A systematic exploration of the observable parameter space On 2010 February 17 we discovered the transient event in the time domain is very likely to lead to many new dis- CSS100217 during the course of the CRTS. This event was coveries (e.g., Djorgovski et al. 2001a, 2001b, and references flagged as unusual at discovery as the object had a past spectrum therein). For example, many types of transient events have been from the SDSS (Abazajian et al. 2009) that resembled a Seyfert, theoretically predicted, yet remain to be convincingly observed. yet the outburst was uncharacteristically rapid and large for an Among these are GRB orphan afterglows (Nakar et al. 2002) AGN. Additionally, there was no detection in archival FIRST and the electromagnetic counterparts to gravitational-wave in- and NRAO VLA Sky Survey (NVSS) radio data covering the spiral events, where close binaries coalesce to release a surge object’s location. The lack of any radio source suggests that the of gravitational radiation (Abadie et al. 2010). Nevertheless, the variability was not being powered by a jet, as seen with optically recent detections of rare types of transients, including candidate variable blazars. Given the unexpected nature of the event, we pair-instability supernovae (Gal-Yam et al. 2010), tidal disrup- immediately scheduled photometric and spectroscopic follow- tion events (TDEs; Gezari et al. 2009a; van Velzen et al. 2010), up of the event. and supernova shock breakouts (Soderberg et al. 2008; Schaw- inskietal.2008) show the promise of current and future large 3. MULTI-WAVELENGTH OBSERVATIONS transient surveys. Following the discovery of the clearly energetic event we Recent optical surveys searching for transient phenomena undertook follow-up observations in X-ray, UV, optical, near- include ROTSE (Akerlof et al. 2000), Sloan Digital Sky Survey IR, and radio wavelengths as well as a targeted archival gamma- (SDSS; Sesar et al. 2007), Palomar Quest (PQ; Djorgovski et al. ray search. In Table 1, we present the sequence and nature of the 2008), the Catalina Real-time Transient Survey (CRTS; Drake follow-up observations we obtained. In the following section et al. 2009), Palomar Transient Factory (PTF; Rau et al. 2009), we will discuss the details of each set of observations as well as and the Panoramic Survey Telescope & Rapid Response System historical data for the source galaxy. We will then combine the (PanSTARRS; Hodapp et al. 2004). In the near future additional data to interpret the nature of the event in relation to known types surveys such as SkyMapper (Keller et al. 2007) and the Large of transients and make concluding remarks about the source. Synoptic Survey Telescope (LSST; Ivezic et al. 2008) will begin operation. At radio wavelengths work is being undertaken by 3.1. UV, Optical, and Near-IR Photometry the low-frequency array (Rottgering 2003), the Allen Telescope Array (Croft et al. 2009) and will soon begin with the Australian Following CSS100217’s discovery, unfiltered observations Square Kilometre Array Pathfinder (Johnston et al. 2007). At continued as part of the CSS survey. All CSS photometry high energies ongoing satellite searches for transients include is routinely transformed to V-magnitudes by using between Fermi 10 and 100 G-type dwarf calibration stars measured in each the Large Area Telescope (LAT; Atwood et al. 2009), 2 Swift Galaxy Evolution Explorer 8deg image.